Development of Kinetic Inductance Detectors in Grenoble Martino - PowerPoint PPT Presentation

Development of Kinetic Inductance Detectors in Grenoble Martino Calvo Institut Néel, CNRS Grenoble

Outline 1 – A ground-based KID instrument: NIKA2 2 – KID for higher frequencies (>300GHz) 3 – KID for lower frequencies (<100GHz) 4 – Getting ready for space... Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 2 2 1 Martino Calvo Kavli IPMU, Japan, 15/12/2015

The IRAM 30m telescope One of the largest single-dish antennas worldwide for the millimetric band 17 arcsec @ 2mm 30 m aperture 12 arcsec @ 1.25mm Correct Field Of View up to 6.5 arcmin 30 m Multi-bands measurements Thousands of ultrasensitive detectors → KID! 1.25mm 2mm A unique tool for Sierra Nevada (Spain) mm-wave astronomy! @2900m a.s.l. Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 3 3 2 Martino Calvo Kavli IPMU, Japan, 15/12/2015

The NIKA2 camera NIKA : the first KID based camera open to external astronomers! NIKA2 : New IRAM KID Array 2 Correct FOV: 6.5 arcmin Total pixel count: ≈ 3000 Arrays count: 3 (2mm + 2 x 1.25mm) The new generation photometric instrument for the 30m telescope Kavli IPMU, Japan, 15/12/2015 On site since last October! (…and for the coming 10 years…) Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 4 4 3 Martino Calvo Kavli IPMU, Japan, 15/12/2015

A NON-space-like cryostat! The cryostat : 1.3 ton 2.3m length Full remote operation Cryogen free Base T ≈ 150mK Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 5 5 4 Martino Calvo Kavli IPMU, Japan, 15/12/2015

A NON-space-like cryostat! The cryostat : 1.3 ton 2.3m length Full remote operation Cryogen free Base T ≈ 150mK The optics : Splitting achieved using quasi-optical elements Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 6 6 4 Martino Calvo Kavli IPMU, Japan, 15/12/2015

A NON-space-like cryostat! The cryostat : Polarizer Dichroic 1.3 ton 2.3m length 1mm V 1mm V Full remote operation 1mm H 1mm H 2mm 2mm Cryogen free Base T ≈ 150mK The optics : Splitting achieved using quasi-optical elements Kavli IPMU, Japan, 15/12/2015 2 colours, + 2 polarizations at 1mm Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 7 7 4 Martino Calvo Kavli IPMU, Japan, 15/12/2015

NIKA2 KID arrays 1000 pixels 2mm array 2mm: 600÷1000 pixels 4 feedlines 2012 JINST 7 P07014 O. Bourrion et al., 1.25mm: 1200÷2000 pixels 8 feedlines Single 4'' wafer fabrication NIKELv1 boards: MUX factor 400 over 500MHz band Kavli IPMU, Japan, 15/12/2015 Current MUX factor: 250 (for safety + Q i on ground!) Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 8 8 5 Martino Calvo Kavli IPMU, Japan, 15/12/2015

The 'house specialty': Hilbert LEKID Hilbert LEKID: a modified version of the standard LEKID design Inductive line based on Hilbert fractal pattern Inductor = radiation absorber! Hilbert LEKID design, 2 -pol M. Roesch et al., Proc ISSTT 2011 Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 9 9 6 Martino Calvo Kavli IPMU, Japan, 15/12/2015

The 'house specialty': Hilbert LEKID Hilbert LEKID: a modified version of the standard LEKID design Inductive line based on Hilbert fractal pattern Inductor = radiation absorber! Need to match Z eff of meander to Z wave Hilbert LEKID design, 2 -pol M. Roesch et al., Proc ISSTT 2011 Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 10 10 6 Martino Calvo Kavli IPMU, Japan, 15/12/2015

The 'house specialty': Hilbert LEKID Hilbert LEKID: a modified version of the standard LEKID design Inductive line based on Hilbert fractal pattern Inductor = radiation absorber! 2mm Need to match Z eff of meander to Z wave Z eff = R □ ∙ (s+w)/w w s High absorption efficiency over large band NIKA2 pixels based on thin film Al ( <20nm ) Hilbert LEKID design, 2 -pol M. Roesch et al., Proc ISSTT 2011 Kavli IPMU, Japan, 15/12/2015 Feedline: CPW or MS Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 11 11 6 Martino Calvo Kavli IPMU, Japan, 15/12/2015

LEKID coupling to radiation Basic principle: Z wave ≈377 W Z eff ≈377 W n=1 n=3.4 Backshort (2n+1) l /4 Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 12 12 7 Martino Calvo Kavli IPMU, Japan, 15/12/2015

LEKID coupling to radiation CPW : back-illumination + Microstrip : front illumination l /4 backshort n=1 Z eff ≈377 W Z eff ≈110 W n=1 n=3.4 l /4 n=3.4 n=1 l /4 Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 13 13 7 Martino Calvo Kavli IPMU, Japan, 15/12/2015

LEKID coupling to radiation CPW : back-illumination + Microstrip : front illumination l /4 backshort AR coating: integrated AR coating: external n=1 Z eff ≈(377/n AR ) W n=1 n eff Z eff ≈110 W n AR n=3.4 l /4 n=3.4 n=1 l /4 BI: ideal for large band applications h > 60% over 100% band FI: ideal for narrower bandwidths Kavli IPMU, Japan, 15/12/2015 h max ≈ 100% at center of 30% band Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 14 14 7 Martino Calvo Kavli IPMU, Japan, 15/12/2015

Lab characterization testbench Available tools allow to fully characterize the arrays: Sky simulator Martin-Pupplet interferometer beam maps/responsivity absorption spectra + radioactive sources & fast electronics Cold BB load → sky Kavli IPMU, Japan, 15/12/2015 A planet ! CR impacts! Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 15 15 8 Martino Calvo Kavli IPMU, Japan, 15/12/2015

Sample array: NIKA2 2mm NIKA2 ' AR11 ' array: 1020 pixels , CPW feedline, AR layer by dicing 4 x 250 pixels, simultaneous readout f shift (Hz) Map of 'planet' (and wire..) >80% good pixels! Kavli IPMU, Japan, 15/12/2015 After removal of doubles and bad KID Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 16 16 9 Martino Calvo Kavli IPMU, Japan, 15/12/2015

NIKA2 arrays on the sky NIKA2 started observations last October For the time being, runs dedicated mainly to commissioning Full operation will start next January 2mm 1.25mm V 1.25mm H Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 17 17 10 Martino Calvo Kavli IPMU, Japan, 15/12/2015

NIKA2 arrays on the sky NIKA2 started observations last October For the time being, runs dedicated mainly to commissioning Full operation will start next January f shift (Hz) (and a real atmosphere...) A real planet! (Uranus) Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 18 18 10 Martino Calvo Kavli IPMU, Japan, 15/12/2015

NIKA2: first light! DR21OH star forming region: ! ! y y r r a a n n i i m m i i l l e e r r P P Integration time: 12 min Kavli IPMU, Japan, 15/12/2015 Credit: N. Ponthieu and NIKA2 collaboration Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 19 19 11 Martino Calvo Kavli IPMU, Japan, 15/12/2015

NIKA2: first light! SZ effect in cluster CLJ1227 ! y r a n i m i l e r P Integration time: 1h06min Kavli IPMU, Japan, 15/12/2015 Credit: F. Ruppin and NIKA2 collaboration Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 20 20 12 Martino Calvo Kavli IPMU, Japan, 15/12/2015

What's next? NIKA2 is up and running... Plenty of good news - it works very well! Results (& papers…) on their way. - experience for detectors in the 100-300GHz range - time to explore something new! Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 21 21 13 Martino Calvo Kavli IPMU, Japan, 15/12/2015

What's next? NIKA2 is up and running... Plenty of good news - it works very well! Results (& papers…) on their way. - experience for detectors in the 100-300GHz range - time to explore something new! 50GHz 100GHz 300GHz 700GHz (luckily enough, choosing ramen is much harder!) Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 22 22 13 Martino Calvo Kavli IPMU, Japan, 15/12/2015

Going to higher frequencies... 50GHz 100GHz 300GHz 700GHz Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 23 23 14 Martino Calvo Kavli IPMU, Japan, 15/12/2015

Going to higher frequencies... Relatively easy to modify LEKID to cover the 300→600GHz range Can keep same technology (eg, materials!) In theory, just need to change the geometry a bit: w, s << l 2mm w s Kavli IPMU, Japan, 15/12/2015 Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 24 24 14 Martino Calvo Kavli IPMU, Japan, 15/12/2015

First test mask for high n LEKID First test mask already made 4 different sub-arrays of 60 pixels each Goal is just a first iteration of the loop design/fabrication/test/feedback! 3.2mm 3.2mm Kavli IPMU, Japan, 15/12/2015 Teaser : pixel size and meander type are not chosen at random! Kavli IPMU, Japan, 15/12/2015 Martino Calvo Martino Calvo 25 25 15 Martino Calvo Kavli IPMU, Japan, 15/12/2015